Strong magnetic fields in supernova remnants (SNRs) are inferred from observations
(e.g., [1]}, [2]}, [3]})
and are also required for confining cosmic ray particles for acceleration.
The above nonlinear dynamo theory has been applied to studying magnetic field amplification in the SNR postshock region in
[4]}.
Different from the interstellar turbulence, the turbulence in the SNR postshock region is driven by the
interaction between supernova shocks and interstellar density inhomogeneities.
The driving scale is comparable to the size of density clumps in the upstream ISM.
